Magnetohydrodynamic properties of extragalactic jets |
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| Authors: | M Nakamura D L Meier D Garofalo |
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| Institution: | (1) Space Telescope Science Institute, Baltimore, MD 21218, USA;(2) Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA;(3) Florida Institute of Technology, Melbourne, FL, USA;(4) European Space Agency, affiliated with the Space Telescope Division of the European Space Agency, ESTEC, Noordwijk, The Netherlands |
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| Abstract: | The theory that magnetic fields are instrumental in the formation and propagation of jets in active galactic nuclei dates
back four decades. Despite a recent growing consensus on this notion stemming from the results of numerical simulations of
magnetohydrodynamic (MHD) flows near black holes, the precise dynamical role of magnetic fields in observed parsec and kiloparsec
jets remains uncertain. Some of the unanswered fundamental questions about extragalactic jets include the location where the
flow becomes relativistic and where acceleration and collimation terminate, as well as the specifics of how the flow interacts
with the ISM. Such observed properties as superluminal motions and wiggled structures based on numerical simulations to constitute
the foundation of an MHD paradigm for extragalactic jets. We particularly focus our attention to the M87 jet, which is one
of the best candidates to investigate relativistic outflows in extragalactic system. |
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